|
 |
The most fundamental property of a star is its mass.
We have seen how mass dictates the evolution of a star,
controlling its lifetime, end state, and which elements it
makes by fusion. So how do we measure mass? The
most fundamental way is to use binary stars: two stars
orbiting each other under their mutual gravitational
attraction. By observing properties of the binary such
as the orbital period and the separation of the stars, we
can learn about the masses of the stars.
About half of the points of light that we see when we look up into the night sky are not single stars
like our Sun but rather the combined light from two or more stars
orbiting each other. For example, the three closest stars to our Sun (remember the parallax and H-R Diagram labs?), alpha Centauri, alpha Centauri-B, and Proxima Centauri are an example of a triple system. |
|